2006/06/28 by David P. Huenemoerder, Paola Testa, Derek L. Buzasi · 3 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Binary number #Binary star #Contact binary #Emission spectrum #Light curve #Polar #Radial velocity #Solar and Space Plasma Dynamics #Spectroscopy #Stars #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/507404
published as Astrophys.J.650:1119-1132,2006 · Accepted for publication in the Astropysical Journal, 23 June 2006; 22 pages, 15 figures
arxiv created 2006/06/28 · openalex publication_date 2006/10/18 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Short-period binaries represent extreme cases in the generation of stellar coronae via a rotational dynamo. Such stars are important for probing the origin and nature of coronae in the regimes of rapid rotation and activity saturation. VW Cep ( P = 0.28 days) is a relatively bright, partially eclipsing, very active object. Light curves made from Chandra HETGS data show flaring and rotational modulation but no eclipses. Velocity modulation of emission lines indicates that one component dominates the X-ray emission. The emission measure is highly structured, having three peaks. Helium-like triplet lines give electron densities of about (3-18) × 10 10 cm -3 . We conclude that the corona is predominantly on the polar regions of the primary star and is compact.